SMR/1847-22 Summer School on Particle Physics 11 - 22 June 2007 SPECIAL LECTURE: Physics at the Weak Scale, Dark Matter and the Matter-Antimatter Asymmetry C.E.M. Wagner EFI, Univ. of Chicago HEP Division, Argonne National Lab. Physics at the Weak Scale, Dark Matter and the Matter-Antimatter Asymmetry C.E.M.Wagner EFI, Univ. of Chicago HEP Division,Argonne National Lab. ICTP Lecture, ICTP, Trieste, Wednesday, June 20, 2007 The new High Energy Physics Framework High Energy Physics has provided an understanding of all data collected in low and high energy collider experiments Contrary to expectations, no signature of physics beyond the SM was observed at the LEP electron-positron collider and no large deviation is being observed at the Tevatron. However, there are two main reasons to believe that there is new physics around the corner. One is related to particle physics, and the other to cosmology: Electroweak Symmetry Breaking Origin of Dark Matter The aim of high energy physics experiments is, in great part, to contribute to the understanding of these two questions. Open questions in the Standard Model Source of Mass of fundamental particles. Nature of the Dark Matter, contributing to most of the matter energy density of the Universe. Origin of the observed asymmetry between particles and antiparticles (Baryon Asymmetry). Dark Energy, Quantum Gravity and Unified Interactions. The Higgs Mechanism and the Origin of Mass A scalar (Higgs) field is introduced. The Higgs field acquires a nonzero value to minimize its energy Spontaneous Breakdown of the symmetry : Vacuum becomes a source of energy = a source of mass 0 <H>< >== v v A physical state (Higgs boson) appear associated to fluctuations in the radial direction . Goldstone modes: Longitudinal component of massive Gauge fields. Masses of fermions and gauge bosons proportional to their couplings to the Higgs field: 2 2 2 2 Mgv2 = g v m = h v m2 = v 2 M WWZ= , ,mtoptop = htoptop vmH =2λv W 2 H What is Dark Matter ? Non-luminous matter that manifest itself via WhatWhatgravitational is is the the interactions Dark Dark Matter Matter ? ? Luminous Matter Luminous Matter Luminous Matter Dark Matter Why do we think that Dark Matter may be accessible at collider experiments ? Dark Matter is most likely associated with new particles Many dark matter candidates have been proposed.They differ in mass and in the range of interaction with SM particles. However, if the relic density proceeds from the primordial thermal bath, there are reasons to believe that it must be part of the dynamics leading to an explanation of electroweak symmetry breaking. It should certainly interact with (annihilate into) ordinary matter at an observable rate ! Evolution of Dark Matter Density d n = 3H n < v >(n 2 n 2 ) , n exp(m/T) dt eff eq eq < > Thermal average of (co-)annihilation cross section eff v n Y = s 3 s g* T Weak-scale size cross sections and masses give the right dark-matter density Dark Matter Annihilation Rate The main reason why we think there is a chance of observing dark matter at colliders is that, when we compute the annihilation rate necessary to obtain the observed relic density, we get a cross section σann.(DM DM → SM SM) 1pb This is precisely 2 αW σann. 2 MW This suggests that it is probably mediated by weakly interacting particles (A.B., K. Matchev and M. Perelstein, PRD 70:077701, 2004) Connection of Thermal Dark Matter to the weak scale and to the mechanism of electroweak symmetry breaking Weak Scale Models and Dark Matter Many different models of particle physics at the weak scale have been proposed Most of them lead to problems of flavor changing transitions or rapid proton decay, unless extra symmetries are invoked These extra symmetries lead to the stability of the lightest new particle, which tend to be neutral and weakly interacting and therefore a good candidate for dark matter I’ll concentrate in the supersymmetric case as a well motivated example of this kind of models. Results from WMAP Universe density 0 = 1.02 ± 0.02 Dark energy density = 0.73 ± 0.04 Total matter density M = 0.27 ± 0.05 Dark matter is non-baryonic Baryon matter density b = 0.044 ± 0.004 Our Universe: us BaryonBaryon Abundance Abundance in in the the Universe Universe Information on the baryon abundance comes from two main sources: Abundance of primordial elements. When combined with Big Bang Nucleosynthesis tell us = n B = 421 , n 3 n cm CMBR, tell us ratio GeV B , 10 5 h2 B c 3 c cm There is a simple relation between these two quantities = 8 2 2.68 10 Bh ElementElement Abundance Abundance and and Big-Bang Big-Bang NucleosynthesisNucleosynthesis predictionspredictions 1GeV 1.6 1024 g Baryon-Antibaryon asymmetry Baryon Number abundance is only a tiny fraction of other relativistic species But in early universe baryons, antibaryons and photons were equally abundant. What explains the above ratio ? No net baryon number if B would be conserved at all times. What generated the small observed baryon-antibaryon asymmetry ? Baryon Number Generation at the Weak Scale (Electroweak Baryogenesis) Baryogenesis at the weak scale Under natural assumptions, there are three conditions, enunciated by Sakharov, that need to be fulfilled for baryogenesis. The SM fulfills them : Baryon number violation: Anomalous Processes C and CP violation: Quark CKM mixing Non-equilibrium: Possible at the electroweak phase transition. BaryogenesisBaryogenesis atat the the Weak Weak Scale Scale Weak scale spectrum and processes to be tested in the near future. Baryogenesis from out of eq. weak scale mass particle decay: Difficult, since non-equilibrium condition is satisfied for small couplings, for which CP- violating effects become small (example: resonant leptogenesis). Pilaftsis,Underwood, hep-ph/0309342 Baryon number violating processes out of equilibrium in the broken phase if phase transition is sufficiently strongly first order: Electroweak Baryogenesis. Cohen, Kaplan and Nelson, hep-ph/9302210; A. Riotto, M. Trodden, hep-ph/9901362 Baryon Number Violation in the Standard Model: Baryon Number conserved at the classical level but violated at the quantum level: Anomaly .. µ B,L N g µ j = Tr() Fµ F µ 32 2 Instanton configurations may be regarded as semiclasical configurationsamplitudes for tunelling effect between vacuum states with different baryon number 2 S = ) inst B0 exp( Sinst W Weak interactions: Transition amplitude exponentially small. No observable baryon number violating effects atT=0 Non-equivalent Vacua and Static Energy in Field Configuration Space The sphaleron is a static configuration with non-vanishing values of the Higgs and gauge boson fields. Its energy may be identified with the height of the barrier separating vacua with different baryon number The quantity v is the Higgs vacuum expectation 8 v value, <H>=v. E = This quantity provides an order parameter which sph distinguishes the electroweak symmetry gW preserving and violating phases. Baryon Number Violation at finite T Anomalous processes violate both baryon and lepton number, but preserve B – L. Relevant for the explanation of the Universe baryon asymmetry. At zero T baryon number violating processes highly suppressed At finite T, only Boltzman suppression Klinkhamer and Manton ’85, Arnold and Mc Lerran ’88 Baryon Asymmetry Preservation If Baryon number generated at the electroweak phase transition, Kuzmin, Rubakov and Shaposhnikov, ’85—’87 Baryon number erased unless the baryon number violating processes are out of equilibrium in the broken phase. Therefore, to preserve the baryon asymmetry, a strongly first order phase transition is necessary: Electroweak Phase Transition Higgs Potential Evolution in the case of a first order Phase Transition Finite Temperature Higgs Potential D receives contributions at one-loop proportional to the sum of the couplings of all bosons and fermions squared, and is responsible for the phenomenon of symmetry restoration E receives contributions proportional to the sum of the cube of all light boson particle couplings Since in the SM the only bosons are the gauge bosons, and the quartic coupling is proportional to the square of the Higgs mass, If the Higgs Boson is created , it will decay rapidly into other particles At LEP energies mainly into pairs of b quarks One detects the decay products of the Higgs and the Z bosons LEP Run is over • No Higgs seen with a mass below 114 GeV • But, tantalizing hint of a Higgs with mass about 115 -- 116 GeV (just at the edge of LEP reach) Electroweak Baryogenesis in the SM is ruled out ElectroweakElectroweak BaryogenesisBaryogenesis andand NewNew Physics Physics at at the the Weak Weak Scale Scale SupersymmetrySupersymmetry fermionsfermions bosonsbosons electronelectron sselectronelectron quarkquark ssquarkquark photphotinoino photonphoton gravitgravitinoino gravitongraviton Photino, Zino and Neutral Higgsino: Neutralinos Charged Wino, charged Higgsino: Charginos Particles and Sparticles share the same couplings to the Higgs. Two superpartners of the two quarks (one for each chirality) couple strongly to the Higgs with a Yukawa coupling of order one (same as the top-quark Yukawa coupling) v2 Two Higgs Doublets necessary: tan β = v1 WhyWhy SupersymmetrySupersymmetry ?? Helps to stabilize the weak scale—Planck scale hierarchy Supersymmetry algebra contains the generator of space-time translations. Necessary ingredient of theory of quantum gravity. Minimal supersymmetric extension of the SM : Leads to Unification of gauge couplings. Starting from positive masses at high energies, electroweak symmetry breaking is induced radiatively. 3B+L+2S If discrete symmetry, P = (-1) is imposed, lightest SUSY particle neutral and stable: Excellent candidate for cold Dark Matter. Preservation of the Baryon Asymmetry EW Baryogenesis requires new boson degrees of freedom with strong couplings to the Higgs. Supersymmetry provides a natural framework for this scenario. Huet, Nelson ’91; Giudice ’91, Espinosa, Quiros,Zwirner ’93. Relevant SUSY particle: Superpartner of the top Each stop has six degrees of freedom (3 of color, two of charge) and coupling of order one to the Higgs M.